Abundance correction differences obtained between the QM and the corresponding EFM (empty circles), DRW, S_H = 0.1 (empty squares) and DRW, S_H = 0.1 collision models (empty triangles), as well as DRW, S_H = 0.002 for Al I, (empty stars) for select Na I, Mg I, Al I and Si I lines, as a function of [Fe/H]. This is shown for the cool giants and dwarfs (left-hand and middle panels), as well as the warm dwarfs (right-hand panels) stellar parameters. The NLTE abundance corrections obtained by the QM models are also shown (filled diamonds), for comparison.